Teilchenteleskope in der Physik - DESYNicht nur Sterne - Gas und Staub. Photons 1 m - 1 km 1 cm 1...

Gernot Maier

Teilchenteleskope in der Physik

Astronomie bei sehr hohen Energien - Gammastrahlungsastronomie

Gernot Maier | Teilchenteleskope in der Physik | October 2010 |

Inhalt

> Astronomie Einführung

Höchste Energien - Gammastrahlung

> Kosmische Teilchenbeschleuniger Explodierende Sterne (Supernovae)

Doppelsternsysteme

Supermassive schwarze Löcher

> Teleskope zur Messung hochenergetischer Gammastrahlung HESS, MAGIC, VERITAS

Fermi - LAT

CTA, AGIS

> Ausblick


Die Milchstrasse

500 Millionen Sterne

100 000 Lichtjahre = 900 000 000 000 000 000 km = 9x1017 km


Die Sonne


Galaxien


Galaxien - Kollisionen


Nicht nur Sterne - Gas und Staub

Photons

1 m - 1 km 1 cm 1 μm - 1 mm 400-700 nm 10 - 400 nm 0.01 - 10 nm < 0.01 nm

Radio

MicrowavesInfrared

VisibleUltraviolet

X-raysGamma-rays

10,000 K 108 K 1010 K

eV keV MeV GeV TeV

1 K 100 K

Photons


Radio

MicrowavesInfrared

VisibleUltraviolet

X-raysGamma-rays

10,000 K 108 K 1010 K

eV keV MeV GeV TeV

1 K 100 K

Charged particles

e±,p

B→

synchrotron radiation

γ γγ’

e±inverse Compton scattering

e±’π0-decay from

hadronic interactions

π0 → γγ

Photons


Radio

MicrowavesInfrared

VisibleUltraviolet

X-raysGamma-rays

10,000 K 108 K 1010 K

eV keV MeV GeV TeV

1 K 100 K

Cosmic Rays (protons, ..., iron nuclei), electrons103 eV 1015 eV 1020 eV

Charged particles

e±,p

B→


γ γγ’




π0 → γγ

Neutrinos

Gravitational waves

Photons


Radio

MicrowavesInfrared

VisibleUltraviolet

X-raysGamma-rays

10,000 K 108 K 1010 K

eV keV MeV GeV TeV

1 K 100 K

Cosmic Rays (protons, ..., iron nuclei), electrons103 eV 1015 eV 1020 eV

Charged particles

e±,p

B→


γ γγ’




π0 → γγ


optical

Multi-wavelength Astronomy


optical

x-ray



infrared

optical

x-ray



Die Milchstrasse

The Milky Way

Optical 0.4-0.6 μm

NASA, mwmw.gsfc.nasa.gov

star light

The Milky Way

Optical 0.4-0.6 μm


star light

thermal emission from interstellar dust

Infrared 12, 60, 100 μm

The Milky Way

Optical 0.4-0.6 μm


very hot, shocked gas

X-ray 0.25, 0.75,1.5 keV

star light



The Milky Way

Optical 0.4-0.6 μm



X-ray 0.25, 0.75,1.5 keV

star light

Hydrogen 21 cm line, cold interstellar medium (gas)

Radio 21 cm



The Milky Way

Optical 0.4-0.6 μm



X-ray 0.25, 0.75,1.5 keV

star light

synchrotron emission from HE electrons moving through interstellar magnetic fields

Radio 480 MHz Hydrogen 21 cm line, cold interstellar medium (gas)

Radio 21 cm



The Milky Way

Optical 0.4-0.6 μm


π0 decay from interaction of Cosmic Rays with interstellar medium

γ-ray >300 MeV


X-ray 0.25, 0.75,1.5 keV

star light



Radio 21 cm



The Milky Way

Optical 0.4-0.6 μm


π0 decay from interaction of Cosmic Rays with interstellar medium

γ-ray >300 MeV


X-ray 0.25, 0.75,1.5 keV

emission from high-energy charged particles>300 GeVγ-ray

star light



Radio 21 cm



InstrumentsArecibo (Radio) Spitzer (IR)Fermi (Gamma-rays)

VERITAS (Gamma-rays)VLT (Optical)

Suzaku (X-rays)

Auger (Cosmic Rays) LIGO (Gravitational waves)

IceCube(Neutrinos)


Radio Microwaves Infrared Visible Ultraviolet X-rays Gamma-rays

10,000 K 108 K 1010 K

eV keV MeV GeV

1 K 100 K

TeV

Gernot Maier | Physics with CTA | October, 2010 |

The non-thermal Universe

TeV

Fermi LAT all sky view > 100 MeV



TeV

sources > 100 GeV



TeV

sources > 100 GeV

Supe

rnova

Remn

ants

Pulsa

r Wind

Nebu

la

Binary

Syste

ms

Starbu

rst Ga

laxies

Activ

e Gala

ctic N

uclei

Gamm

a Ray

Burst

s

Dark

Matte

r



TeV

sources > 100 GeV

Supe

rnova

Remn

ants

Pulsa

r Wind

Nebu

la

Binary

Syste

ms

Starbu

rst Ga

laxies

Activ

e Gala

ctic N

uclei

Gamm

a Ray

Burst

s

Dark

Matte

r

500 Million stars known in the Milky Way 100 very high-energy gamma-ray sources known


Quellen von Gammastrahlung - Explodierende Sterne

Massive Sterne explodieren am Ende ihres ‘Lebens’

Wahrscheinlich die Quellen der kosmischen Strahlung

Tycho’s Supernova (1572)

Teilchenbeschleunigung

heißer Überrest (Millionen Grad Celsius)

• distant bright galaxies

• central core produces more radiation than rest of galaxy: Active Galactic Nucleus (AGN)

• supermassive black hole: 109 solar masses

• extremely powerful radio source: quasar

• ~10% of all AGNs produce beams of energetic particles and magnetic fields: jets

• powered by accretion of matter onto a supermassive black hole and/or black hole rotation

M87: HST opticalActive Galactic Nuclei

core and accretion disk

jet: relativistic, hot, magnetized plasma

thou

sand

s of l

ight

year

s

hot spots: shocked jet

plasma

blue light: synchrotron radiation from HE

electrons

• distant bright galaxies

• central core produces more radiation than rest of galaxy: Active Galactic Nucleus (AGN)

• supermassive black hole: 109 solar masses

• extremely powerful radio source: quasar

• ~10% of all AGNs produce beams of energetic particles and magnetic fields: jets

• powered by accretion of matter onto a supermassive black hole and/or black hole rotation


core and accretion disk

jet: relativistic, hot, magnetized plasma

thou

sand

s of l

ight

year

s

hot spots: shocked jet

plasma

blue light: synchrotron radiation from HE

electrons



Schwarze Löcher und Jets

HH30: 1995 - 2000

SS 433(2-10 keV)

Young Stars(Herbig-Haro Objects)

Microquasars(X-ray binaries)

Gamma Ray Bursts(hypernovae)

long GRBscollapse of massive, rapidly rotating stars


Quellen von Gammastrahlung - Doppelsternsysteme

Mikroquasar


Quellen von Gammastrahlung - Doppelsternsysteme

Mikroquasar

accretion disk

jet

core: black hole or neutron star

donor star

Charged Particle Acceleration - Shocks in the Universe

kitchen sink Kepler’s Supernova

Extragalactic background light:How many stars are in the sky?

γTeV+γstar → e+e-


Dark Matter

Atoms4%

Dark Matter26%

Dark Energy70%

Wir kennen nur 4% unseres Universums...


Dark Matter

Galactic center

Dwarf Galaxies

Milky Way Halo


The non-thermal Universe - the big questions

TeV

Supe

rnova

Remn

ants

Pulsa

r Wind

Nebu

la

Binary

Syste

ms

Starbu

rst Ga

laxies

Activ

e Gala

ctic N

uclei

Gamm

a Ray

Burst

s

Dark

Matte

r



TeV

Supe

rnova

Remn

ants

Pulsa

r Wind

Nebu

la

Binary

Syste

ms

Starbu

rst Ga

laxies

Activ

e Gala

ctic N

uclei

Gamm

a Ray

Burst

s

Dark

Matte

r

Understanding the origin of cosmic rays and how they interact with their environment.



TeV

Supe

rnova

Remn

ants

Pulsa

r Wind

Nebu

la

Binary

Syste

ms

Starbu

rst Ga

laxies

Activ

e Gala

ctic N

uclei

Gamm

a Ray

Burst

s

Dark

Matte

r

Understanding the nature and variety of black hole particle accelerators.




TeV

Supe

rnova

Remn

ants

Pulsa

r Wind

Nebu

la

Binary

Syste

ms

Starbu

rst Ga

laxies

Activ

e Gala

ctic N

uclei

Gamm

a Ray

Burst

s

Dark

Matte

r

What is the nature of dark-matter particles?

Understanding the nature and variety of black hole particle accelerators.


VHE Cherenkov telescopes

VERITAS

MAGIC

H.E.S.S.

Cangoroo

Fermi LAT

Whipple

VERITAS

H.E.S.S.


October 1968

First detection:1989


A CTA telescope


Atmospheric Opacity

e+

e–

e–

e–

e+ e+

e

p

e–

v~

ca. 100-200m

Extensive Air Showers

prim

ary

part

icle

primaryparticle

show

er a

xis

lead

ing

hadr

on

e/ detector arrayhadroncalorimeter

fluorescence,cherenkov light

! detectors

~1 m thick

composition of part.at ground level(after 25 X0, 11 int)

! 80 % photons! 18 % electrons! 1.7 % muons! 0.3 % hadrons! 106 secondary part. from 1015 eV proton

~ 20km height

c


Cherenkov light

Pavel Alekseyevich Cherenkov(Nobel 1958)

emitted when velocity of charged particle exceeds local speed of light


Detection of high-energy γ-rays

γ-ray

particle shower

~10 km

‘flat’ light pool with radius of ~120 m:

detection areas of 105 to 106 m2

Cherenkov photon densities on ground level:

1-105 γ/m2

duration of Cherenkov flash: ~ns


Fluxes

> flux of strongest γ-ray source (Crab Nebula): ~10-7 γ’s/m2/s

>satellite with detection area of 1-5 m2: ~15 γ’s / year

> imaging atmospheric Cherenkov telescopes: detection area >105 m2: 50 γ’s/h

Power law E-2.4

Background

γ-ray proton

Cosmic Ray flux typically 103-104 larger than γ-ray flux

Background

γ-ray protonCherenkov photons on ground

γ-ray

proton

Cosmic Ray flux typically 103-104 larger than γ-ray flux

shower

maximum at8-10 km altitude

alti

tude

Cherenkov flash is a few nanoseconds long

shower


alti

tude

mirror


shower


alti

tude

focal plane

mirror


shower


alti

tude

Image in the focalplane

focal plane

mirror


(observation of the Crab Nebula)gamma-rays measured by VERITAS

(each frame 2 ns long)

Monte Carlo Simulation

gamma-rays ‘measured’ by VERITAS

(each frame 2 ns long)


VERITAS - Technical Details

Telescope (x 4)12 m diameter Davies-Cottonf 1.0, 110 m2 mirror area

Mirror Facets (x 350)Reflectivity ~88%(recoated every 2 y) Light concentrators

3.5°

Camera (x 4)499 PMTs3.5o Field of View

PMT (x 499)

FADC SAMPLES

Electronics500 MSPS FADCCFD trigger,3 adjacent pixel and 2/4 telescope coincidence~10% dead time; ~300 Hz

Pointing Monitor


The Cherenkov Telescope Array

CTA Consortium: >22 countries (big: D, F, US) >600 scientists€180 M (invest)first science data 2014

north and south array - full sky coverage


The Cherenkov Telescope ArrayCrab

10% Crab

1% Crab

FERMI LAT

MAGIC

H.E.S.S./VERITAS

CTA

CTA Consortium: >22 countries (big: D, F, US) >600 scientists€180 M (invest)first science data 2014

north and south array - full sky coverage

Teilchenteleskope in der Physik - DESYNicht nur Sterne - Gas und Staub. Photons 1 m - 1 km 1 cm 1...

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